Tuesday, March 31, 2009

Would young people learn science betterif it were packaged in a videogame?

That's the question at the heart of the Selene project, originally funded by NASA and carried through a four-year grant from the NSF. Selene studies video game learning and the ways researchers can assess how effectively that learning takes place.

Selene challenges players to learn the major geologic processes scientists believe formed the modern Moon. Players create their own moon and then pepper it with impact craters and flood it with lava. It's a great opportunity for students to learn about lunar geology while helping researchers study some key videogame design principles. In addition, playing Selene offers a way to take part in the International Year of Astronomy 2009, a global celebration of astronomy and its contributions to society and culture, highlighted by the 400th anniversary of the first use of an astronomical telescope by Galileo Galilei.

CET's research project CyGaMEs uses Selene to introduce players ages 13-18 the Moon's geology and researchers track players' game-play to study how Selene helps players to pick up on that subject matter. Developers currently have the project aligned to National Science Standards and the Texas State Science Standards. Other states standards are currently being developed.

CET presents numerous opportunities for educators to become involved, including working on game design, development, collaborative research and utilizing the project with students.

The Center for Educational Technologies produced Selene to conduct its research. If you're a student between the ages of 13-18, we'd love to have you play. The game takes about an hour to complete, but you can spend more time after checking out Selene's various resources about the Moon. To play, though, you have to be enrolled by an adult recruiter to ensure parent/guardian consent for your participation.

If you're an adult who'd like to help out, click on the Recruiter button at left and help us find players to take part in the study. Being a recruiter is simple and doesn't involve a lot of paperwork. The whole process involves getting oral consent from a parent or guardian, then forwarding Selene registration access to your recruited players. It's that simple.

Join in this exciting venture and be a part of cutting-edge research sponsored by the National Science Foundation.

NASA showcased the Orion command module, Monday in a day-long public event on the National Mall in Washington. The full-size mockup of the Constellation CEV was parked on the Mall between 4th and 7th Streets, SW, in front of the National Air and Space Museum. Reporters attended a briefing Monday morning.

The spacecraft mockup is on its way from water testing at the Naval Surface Warfare Center's Carderock Division in Bethesda to open water testing in the Atlantic, off the coast of KSC.

The goal of the operation, dubbed the Post-landing Orion Recovery Test, or PORT, is to determine what kind of motions the astronaut crew can expect after landing, as well as conditions outside for the recovery team.

Orion is targeted to begin carrying humans to ISS no sooner than 2015 and to the moon in 2020.

In this paper we present a new method for dating the surface of the Moon, obtained by modeling the incoming flux of impactors and converting it into a size distribution of resulting craters. We compare the results from this model with the standard chronology for the Moon showing their similarities and discrepancies. In particular, we find indications of a non-constant impactor flux in the last 500 Myr and also discuss the implications of our findings for the Late Heavy Bombardment hypothesis. We also show the potential of our model for accurate dating of other inner Solar System bodies, by applying it to Mercury.

Les Mureaux - March 31 (Reuters) - Astrium, the space unit of aerospace group EADS, says it is seeking support to build two extra resupply vehicles worth 400 million euros for the International Space Station.

The first ATV (Automated Transfer Vehicle) Jules Verne docked with ISS last year and was a breakthrough for the European Space Agency.

"We have sent ESA an offer to build two extra ATVs," Alain Charmeau, head of Astrium Space Transportation, told reporters, adding he expected to get a response by the end of 2009.

ESA was not immediately available to comment.

Ministers from the 18-nation ESA agreed in November to develop a new version of the ATV that would return cargo from the space station to Earth without burning up in the atmosphere.

Description: It all started with the second person who created a lunar map. Naming features on the Moon has had a long and contentious history. The various lunar maps, sketches and images produced during the last four centuries show how difficult it can be to be accurate and consistent in lunar nomenclature. Amateur astronomer 'Lunar Mark' Tillotson talks about some of the major selenographers and the people who are honored with a lunar feature.

Bio: Mark Tillotson is an engineer and amateur astronomer living in Pennsylvania. He is interested in the Moon, the history of astronomy and science in general. Mark is the author of two blogs, Today in Astronomy and Lunar Mark, and created the Astronomy Compendium; a wiki-spaces site designed as a collection of information about the people, places and events that shaped the science of Astronomy into the form we know today. He is the Star Party coordinator at the Lehigh Valley Amateur Astronomical Society and a communications team member for IYA2009 US; posting updates on Facebook as IYA Cosmos and on Twitter as IYA.

Last week, four Spanish students revealed how they had taken pictures of the curvature of the Earth by attaching a digital camera to a helium balloon and letting it go. When the British newspaper The Daily Telegraph reported the work, the story snowballed, attracting worldwide coverage.

Now a group of 30 Italian students from classes 1SD and 1SE at the Liceo Scientifico "A. Vallisneri" in Lucca, Italy have gone one better with an ingenious measurement of the distance to the moon.

The students analysed an mp3 recording of the conversation between Neil Armstrong on the surface and ground control in Houston in which he utters his famous "one small step" speech. The recording is available on the NASA website.

They noticed an echo on this recording in which sentences from Earth are retransmitted via Armstrong's helmet speaker through his microphone and back to Earth. They used the open source audio editing program Audacity to measure the echo's delay which turned out to be 2.620 secs and used this to work out the distance to the moon as 3.93 x 10^8 metres.

That's not bad given that the actual distance varies between 3.63 and 4.05 x10^8 metres.

The students then went on to measure the eccentricity of the moon's orbit using conversations recorded during the Apollo 17 mission, which was on the lunar surface for 300 hours.

They even estimated their errors using the Moon's ephemerides. Likely errors include delays caused by electronics and the time it took for the signals to be routed to the various antennae around the world that NASA used for communications.

The man in the moon always presents us with the same mugshot, because the Earth's tides have locked the moon's spin to ours. But in a talk yesterday, Mark Wieczorek pointed out that not only did it not always have to be this way, but also that there is some evidence that the moon actually did swap its Earth-facing side at least once in the ancient past.

The work builds on a theoretical result in the 1970s from the University of Arizona's Jay Melosh, who showed that there were two equally stable ways in which the face of the moon could freeze toward Earth: the near side, and the far side. A glancing blow from a moderately big asteroid would be enough to do the job. Wieczorek, of the Institut de Physique du Globe de Paris, now shows that if that was the case, there would be a slight preponderance of big impacts on the moon's leading edge (marked 'apex' in the image here), since its orbiting velocity would be added to, rather than subtracted from, the impacting object. Lo and behold, he finds, the oldest impacts cluster around the moon's trailing face -- implying a flip-flop. "It's probably happened several times," he says. Most basin impacts would be big enough for the great switcheroo, but based on chronology, Wieczorek suggests that Smythii would be a likely candidate.

He says the process of a face switch could even start and stop temporary lunar dynamos -- which would be an interesting new mechanism for imprinting magnetic orientations onto lunar rocks.

Melosh was pleased that someone followed up on his theoretical idea, and says it needs to be tested on many of the Jovian and Saturnian satellites. "This suggests that this could be a common process with the other tidally locked satellites," he says.

Jacobsen, Remo, Petaev & Sasselov: Hf-W Chronometry and the Timing of the Giant Moon-forming Impact on Earth[#2054] For Hf-W chronometry of the Earth-Moon system (EMS) there are currently two end member options: (i) the formation of the EMS at ~32 Myr or (ii) formation of 90% of the Earth in the first six Myr followed by a very late (~100 Myr) formation of the Moon.

Touboul, Kleine, Bourdon, Nyquist & Shih: New 142Nd Evidence for a Non-Chondritic Composition of the Moon[#2269] Here we present new Sm-Nd data for lunar rocks that are used to evaluate the significance of the 146Sm-142Nd systematics for constraining the timescale of lunar differentiation and the bulk Nd isotope composition of the Moon.

Pahlevan & Stevenson: Chemical Fractionation after the Moon-forming Giant Impact[#2392] We test the hypothesis that the lunar mantle is derived from the terrestrial mantle via liquid-vapor fractionation during the afterglow of the giant impact.

Zindler & Jacobsen:Isotopic Equilibration of Earth’s Mantle and the Moon Subsequent to the Giant Impact?[#2542] The striking oxygen, chromium, and tungsten isotopic similarities between the Earth’s mantle and the Moon are discussed and modeled with a 3-box model.

E.M. Parmentier: On the Scale of Lunar Mantle Overturn Following Magma Ocean Fractional Solidification: The Role for Multiple Scales of Convective Motion[#1781] Multiple scales of mantle overturn following magma ocean fractional solidification reconciles the magmatic evolution of the Moon many of its important geological and geophysical characteristics.

J. Longhi: Origin of the Magnesian Suite Cumulates[#2356] Melting calculations on various combinations of rock types formed in the lunar magma ocean suggest that highly magnesian olivine characteristic of magnesian suite cumulates ultimately derives from the earliest dunite cumulates of the magma ocean.

Grange, Nemchin, Pidgeon & Meyer: Early History of the Moon: Zircon Perspective[#1473] U-Pb ages of lunar zircons highlight new details in the early history of the Moon, providing a younger limit for the LMO crystallization and indicating that the impact history of the Moon is more complex than the accepted late period of bombardment.

H.V. Frey: Crustal Thickness Evidence for More Previously Unrecognized Large Lunar Basins[#1687] Crustal thickness model data reveal the presence of even more large lunar basins that were previously unrecognized. The total number of lunar basins >300 km diameter may exceed 150, more than three times that determined by photogeologic mapping alone.

Wieczorek & Le Feuvre: Did a Large Impact Reorient the Moon?[#1554] More impacts should occur on the Moon’s western hemisphere as a result of this body’s synchronous rotation. We show that there are more old basins located on the Moon’s eastern hemisphere, suggesting that a large impact reoriented the Moon by 180°.

Cahill, Lucey & Wieczorek: The Composition of Lunar Central Peaks Relative to Lunar Samples[#1222] Here we place the modeled mineralogy of lunar impact crater central peaks in the context of the lunar sample collection.

Wingo & Cowing: Recovering High Resolution Lunar Orbiter Images from Analog Tape [#2517] Original FR-900 tape recorders have been refurbished to play, digitize, and store, the original highest resolution images of the Moon. This paper outlines the process and the initial results of our efforts.

Tuesday, March 24, 2009

SPECIAL SESSION:LUNAR MISSIONS: RESULTS FROM KAGUYA, CHANG’E-1, AND CHANDRAYAAN-1

PART ONEChairs: Clive Neal & Alian Wang

Goswami & Annadurai: Chandrayaan-1: India’s First Planetary Science Mission to the Moon[#2571]The first Indian planetary exploration mission, Chandrayaan-1, was launched on 22 October, 2008. We will present a brief summary of the science objectives, various payloads, mission details and observational plans.

Dachev, Tomov, Matviichuk, Dimitrov, Angelis, Spurny, & Vadawale: Monitoring of the Earth and Moon Radiation Environment by the RADOM Instrument on Indian Chandrayyan-1 Satellite. Preliminary Results [#1274]This paper describes preliminary scientific results from the measurements of the Earth and Moon radiation environment by RADOM instrument since 22nd October 2008.

De Angelis, Dachev, Tomov, Matviichuk, Dimitrov, Spurny & Vadawale: Modeling of the Moon Radiation Environment at the Altitude of the Indian Chandrayaan-1 Satellite and a Comparison with the RADOM Experiment Data [#1310] These results for the moon radiation environment as well as for the cruise phase have been obtained in the framework of the Radom investigation that is on-board the Chandrayaan-1 mission by the Indian Space Agency ISRO.

Spudis, Bussey, Butler, Carter, Gillis-Davis, Goswami, Heggy, Kirk, Misra, Nozette, Robinson, Raney, Thomson & Ustinov: The Mini-SAR Imaging Radar on the Chandrayaan-1 Mission to the Moon [#1098] The Mini-SAR is an imaging radar instrument on the Indian Chandrayaan-1 mission to the Moon. It will map both lunar poles, revealing terrain in permanently dark areas and characterizing the backscattering properties of these areas, looking for evidence of ice.

Pieters & Moon Mineralogy Mapper Team: Mineralogy of the Lunar Crust in Spatial Context: First Results from the Moon Mineralogy Mapper (M3)[#2052]Mineralogy across the Orientale Basin measured with initial M3 data indicate the peak ring exposed a massive crustal layer of almost pure anorthosite. This is underlain by noritic materials. More mineralogy data of the lunar crust is being acquired.

Namiki, et.al.: Comparative Study of Compensation Mechanism of Lunar Impact Basins from New Gravity Field Model of SELENE (Kaguya)[#1519] Based on the gravity model of the Moon by SELENE, we propose new classification and compensation mechanism of lunar impact basins. Impact basins on lunar far side are classified into two types depending on free-air and Bouguer gravity anomalies.

Ishihara, et.al.:Localized Gravity/Topography Correlation and Admittance Spectra on the Moon[#1623] We show the results of localized correlation and admittance analysis using new lunar gravity and topography models from Kaguya mission.

Araki & Tazawa, et.al: The Lunar Global Topography by the Laser Altimeter (LALT) Onboard Kaguya (SELENE): Results from the One Year Observation[#1432] A global and precise topographic map of the Moon has been derived by the laser altimeter (LALT) onboard the Japanese lunar explorer Kaguya (SELENE). Results of the one year observation and implications from the LALT topography will be presented.

Honda & Yamazaki - Mitsuhashi, Tachino, Yamauchi & Shirao: Results of High-Definition Television System (HDTV) On Board SELENE (Kaguya)[#2540] The current status of the HDTV, recent data obtained, and ongoing data analysis of HDTV images such as the creation of digital elevation model (DEM) from the moving images are reported.

Hirata, et.al.: Morphological Analyses of Tycho Crater with Kaguya Data[#1514] We investigated a large lunar crater Tycho with Kaguya/LISM data to reconstruct the impact event forming the crater from distributions of its ejecta and other associated features.

Okumura H. Sobue S. Hoshino H. Yamamoto A. Fujita T. Data Archive and Visualization for Lunar Orbiter Kaguya (SELENE) [#1518] Kaguya Data Archive (L2DB) and Kaguya Web Map Server(WMS) are being developed in JAXA Sagamihara Campus and will be open to the public from Nov. 2009. Also World Wind for Kaguya and KML data set will be prepared for the purpose of research and EPO.

Taylor L. A. Liu Y. Pieters C. Tompkins S. Isaacson P. Cheek L. Thaisen K. Lunar Magma Ocean Crust: Implications of FeO Contents in Plagioclase[#1304] The FeO and MgO compositions of the highland plagioclase, particularly that in the FANs, do not represent those from the original LMO. The re-equilibrated values are due to slow cooling of the proto-crust, similar to anorthosites on Earth (Phinney, 1991).

Pieters C. Kumar S. Head J. W. Goswami J. N. Kumar K. Green R. Boardman J. Staid M. Petro N. Isaacson P. Lunar Orientale Basin: Nature of Impact Melt and Volcanic Flooding from Chandrayaan-1 (M3, TMC, HySI)[#2157] A subset of data observed by M3, TMC, and HySI is used to evaluate the relation of the Maunder Formation and neighboring basalts. The MF is shown to be highly feldspathic and the basalts exhibit features suggestive of magma movement during cooling.

de Vries J. van den Berg A. P. van Westrenen W.The Formation and Evolution of a Lunar Core from Ilmenite-rich Magma Ocean Cumulates[#1244] The possibility of forming an ilmenite-rich core in the moon is studied, using numerical models. It is shown that core density and sharpness of the core-mantle boundary depend on the heat production in and the density of the ilmenite-rich material.

Sakai R. Kushiro I. Nagahara H. Ozawa K. Tachibana S.Experimental Constraints on Composition of Lunar Magma Ocean from Physical Properties of Magma[#1839] We performed high-pressure experiments to determine density and viscosity of magma with chemical compositions plausible to the anorthosite crust formation in order to put physical and chemical constraints on differentiation of the lunar magma ocean.

Bauch K. E. Hiesinger H. Helbert J. Estimation of Lunar Surface Temperatures: A Numerical Model [#1789] We present global temperature estimates for sunrise, noontime and sunset. This work provides new and updated research on the temperature variations by taking into account the surface and subsurface bulk thermophysical properties.

Weber R. C. Bills B. G. Johnson C. L. A Simple Physical Model for Deep Moonquakes[#1870] Tidal stress is widely believed to influence the occurrence times of deep moonquakes. We explore several simple models of stress buildup and release that can be used to create moonquake-like time sequences of events.

Kawamura T. Tanaka S. Saito Y. Kobayashi Y. Horai K. Hagermann A. Re-Determination of Deep Moonquake Sources Using the Apollo 17 Lunar Surface Gravimeter [#1653] We performed the first seismic analysis of deep moonquakes using the Apollo 17 Lunar Surface Gravimeter. We re-determined the seismic source of the deep moonquakes and evaluated the contribution of the LSG.

Mazarico E. Han S.-C. Lemoine F. G. Smith D. E.A New Solution of the Lunar Gravity Field Using Localized Spectral Constraint [#2248] We use localized spherical harmonics to create a lunar gravity field solution with the Kaula constraint applied only to the far side. The differences with a globally constrained solution are correlated with the topography, suggesting an improvement.

de Meijer R. J. van Westrenen W. An Alternative Hypothesis for the Formation of the Moon[#1847] We propose an alternative explanation for the compositional correspondence between Moon and silicate Earth: the Moon formed from the ejection of terrestrial mantle material, triggered by a run-away natural georeactor at Earth’s core-mantle boundary.

Chevrel S. D. Pinet P. C. Daydou Y. Le Mouélic S. Langevin Y. Costard F. Erard S. The Aristarchus Plateau on the Moon: Nature and Stratigraphy of the Substratum[#1234] From Clementine UVVIS and NIR spectral data, a statistical analysis and a mixture modeling, we present the mineralogy and the stratigraphy of the materials forming the substratum and volcanic deposits of the Aristarchus Plateau on the Moon.

Weider S. Z. Crawford I. A. Joy K. H.Investigating Oceanus Procellarum Basalt Flows Using Integrated Clementine UV-VIS and NIR Data[#1573]We use UV-VIS and NIR data from Clementine to investigate the basaltic stratigraphy in a region of Oceanus Procellarum. This enables us to study the FeO and TiO2 compositions, major mafic mineralogy, and extent of spaceweathering of these deposits.

Srivastava N. Spectral Reflectance Studies for Maturation Trends in a Mare and Highland Swirl[#1577] Regions shielded by maximum magnetic field intensity in the proto type swirl Reiner Gamma and the one near Airy Crater, have been investigated for maturity trends. Both the cases show differences (though of reversed nature) from the trend seen in nearby unshielded areas.

FuPing G. YanMei Y. Geological Features Study of the Lunar Surface Using the Lunar Remote Sensing Data[#1457] Taking typical craters of lunar surface as the test areas, using the Clementine UVVIS, NIR and lidar data, we study the relationship between the geological features and physiognomy, analyze the rule of lithology or mineral distribution of the lunar.

Aarthy R. S. Sanjeevi S. Vijayan S. Krishnamurthy J.Spectral Studies of Anorthosite and Meteorite[#2216] The aim of this study is for the better understanding of the lunar highland surface. Thus for the study anorthosite and meteorite (not yet being approve) spectral studies were carried out.

Stockstill-Cahill K. R. Cahill J. T. S. Lucey P. G. Hawke B. R. Radiative Transfer Modeling of Lunar Hyperspectral Data[#1629] We have previously developed multispectral methods for deriving minerals from spectra. We are now extending these methods to continuous (hyperspectral) telescopic data for various locations on the nearside of the Moon.

LRO AND LCROSS

Mazarico E. Neumann G. A. Rowlands D. D. Lemoine F. G. Smith D. E. Zuber M. T. Multi-Beam Altimetric Crossovers for the Precision Orbit Determination of the Lunar Reconnaissance Orbiter [#2244] We study a new type of altimetric crossovers enabled by LOLA multi-beam configuration. Those use the cross-track information and can help the LRO goal of creating a new lunar reference frame by providing stronger constraints on the orbit.

Thomas I. R. Bowles N. E. Greenhagen B. T. Reflectance and Emission Measurements of Lunar Analogues for Interpretation of Returning Data from the Diviner Lunar Radiometer on NASA’s Lunar Reconnaissance Orbiter (LRO)[#2110] In support of the Diviner Compositional Investigation, spectra of many lunar analogues were measured from UV/VIS to FIR. Reflectance and emission spectra were found for samples with differing mineralogy and grain size, in various atmospheric pressures.

Heldmann J. L. Colaprete A. Wooden D. Asphaug E. Schultz P. Plesko C. S. Ong L. Korycansky D. Galal K. Briggs G.Lunar Crater Observation and Sensing Satellite (LCROSS) Mission: Opportunities for Observations of the Impact Plumes from Ground-based and Space-based Telescopes[#1898]The primary objective of the LCROSS mission is to investigate the presence or absence of water on the Moon. Ground-based and orbital observatories can observe the dust and water vapor plume caused by the two impacts into the lunar surface.

Bart G. D. Colaprete A. Shadow Depths and Other Characteristics of Potential LCROSS Impact Sites[#2151]LCROSS impact site selection is critical to mission success. We discuss the critical constraints site selection, the ongoing work to characterize potential sites, and the most recent work of determining shadow depths at potential impact sites.

Summy D. Goldstein D. B. Colaprete A. Varghese P. L. Trafton L. M. LCROSS Impact: Dust and Gas Dynamics [#2267] We present results from simulations of the plume resulting from the impact of the LCROSS vehicle(s) into a shadowed lunar polar cold trap. Results may be of particular interest to those planning observations of the H2O, OH and dust plumes.

Hermalyn B. Schultz P. H. Heineck J. T. LCROSS Early-Time Ejecta Distribution: Predictions from Experiments[#2416] Experimental results of the early-time ejecta distribution from impacts of projectiles with a range of relative densities are presented, with implications and predictions for the upcoming LCROSS mission.

Thursday, March 26, 2009POSTER SESSION 2:PURSUING LUNAR EXPLORATION

Wilson T. L. Lee K. T. Photon Luminescence of the Moon[#1918]The space-radiation-induced photon luminescence existing on the Moon is derived from SEP and GCR sources. Its spectrum is present in the upper X-ray and lower γ-ray portion of the electromagnetic spectrum. Dose mitigation measures are addressed.

Petro N. E. Bleacher J. E. Clark P. E. Mest S. C. Lewis R. Optimizing Lunar Surface Science: Comparison of Shackleton Base Scenario and Sortie Surface Scenarios at the Nectaris Basin, Marius Hills, and Olivine Hill[#2206] The work reported here responds to the need to provide the Constellation program with science requirements for a surface system architecture and metrics for surface operations. We compare surface scenarios for an outpost at Shackleton to three sorties.

Ruberg R. Wood C. A. Reese D. D. Lightfritz C. Harrison A. MoonWorld: Virtual Fieldwork in Second Life[#2229] MoonWorld is a Second Life simulation that models the Moon as a tool for learning lunar science through virtual fieldwork. Avatars climb into craters to collect samples and observe structure to understand crater formation.

Boldoghy B. Kummert J. Varga T. P. Szilágyi I. Darányi I. Bérczi Sz. Varga T. N. Hudoba G. Jr. Buildings of Great Inner Space Created with Low Asset Requirement and High Efficiency for the Moon[#2458] For constructing lunar base buildings of great inner space we propose a plan, architectural concept, and building technology of using local materials by various technologies, baking, bagging and moving of the regolith to cover the building.

Burger P. V. Shearer C. K. Papike J. J.The Multi-Stage Cooling History of Lunar Meteorite NWA 032 as Recorded by Phenocrystic Olivine and Pyroxene[#2043] This study examines previously undocumented oscillatory zoning in phenocrystic pyroxene grains from lunar meteorite NWA 032, and its implication for the crystallization history of this sample.

Hauri E. H. Saal A. E. Van Orman J. Rutherford M. J. Friedman B. New Estimates of the Water Content of the Moon from Apollo 15 Picritic Glasses [#2344] In this abstract, we report the results of new SIMS measurements of water on over 200 new samples of picritic glasses recovered from the Apollo 15 mission. Our new measurements suggest an upward revsion of current estimates for the water content of lunar magmas.

Wilson L. Head J. W. Lunar Volcanic Eruptions: Range of Eruption Styles and Implications for Magma Ascent and Emplacement[#1159] We characterize the range of volcanic feature morphologies observed on the Moon in a manner suitable to allow them to be related to the conditions under which eruptions and intrusions took place.

CHEMICAL AND PHYSICAL PROPERTIES OF THE LUNAR REGOLITH

Spudis P. D. Taylor G. J. A Major KREEP-Basalt — Mare Basalt Unconformity on the Moon[#1039] The Station 2 boulder at Apollo 15 preserves a major 500 Ma unconformity between early Imbrian-age non-mare KREEP basalts and late Imbrian-age mare basalt. These samples may represent a paleoregolith, an ancient regolith preserved between two lava flows on the Moon.

McKay D. S. Cooper B. L. Riofrio L. M. New Measurements of the Particle Size Distribution of Apollo 11 Lunar Soil [#2051] We have initiated a major new program to determine the grain size distribution of nearly all lunar soils collected in the Apollo program. The use of a laser diffraction instrument improves upon previous work using sieving.

Edmunson J. Cohen B. A. Spilde M. N. Characterizing the Effect of Shock on Isotopic Ages I: Ferroan Anorthosite Major Elements[#2094] Ferroan anorthosites 62236 and 67075 do not show major element mobility due to shock in microprobe analysis. The shock pressure of 67075 is estimated at <50>

ten Kate I. L. Glavin D. P. VAPoR Team Evolved Gas Analysis of Two Lunar Simulants, Apollo 16 Regolith and a Carbonaceous Meteorite (Murchison) Using VAPoR[#2232] Volatile Analysis by Pyrolysis of Regolith (VAPoR) on the Moon using mass spectrometry is one technique that should be considered for in situ analysis of lunar regolith. Here we present evolved gas analysis data obtained with the VAPoR breadboard.

Wilson T. L. Lunar Dust and Dusty Plasma Physics[#1314] Lunar dust is addressed using the physics of dusty plasmas. Equations for small dust grains on the Moon are given and related to MHD effects of plasma precipitation as it orbits through the Earth’s plasma sphere, magnetosphere, and the solar wind.

Cook A. C. Grande M. Preliminary Analysis of Transient Lunar Phenomena Catalog Data[#2429] We have completed a new catalog of Transient Lunar Phenomena and have performed an initial statistical analysis on this.

Archinal B. Lunar Geodesy and Cartography Working Group Activities of the NASA LPRP Lunar Geodesy and Cartography Working Group[#2095] We describe the purpose, operation, activities, and future plans of the NASA Lunar Precursor Robotic Program Lunar Geodesy and Cartography Working Group. New standards/recommendations and the need to geodetically control lunar datasets are examined.

Williams D. R. Schultz A. B. Hills H. K. Guinness E. A. Lowman P. D. Taylor P. T.Restoration of Apollo Data by the PDS Lunar Data Node[#1991] The Lunar Data Node (LDN) has been formed to put relevant, scientifically important Apollo data into accessible digital form for use by researchers and mission planners. We will report on progress made since last year and plans for future data restorations.

Lee E. M. Gaddis L. R. Weller L. Richie J. O. Becker T. Shinaman J. Rosiek M. R. Archinal B. A. A New Clementine Basemap of the Moon[#2445] The new basemap of the Moon based on ULCN2005 will be distributed through USGS Map-A-Planet web site (http://www.mapaplanet.org). The image geometry was verified for accuracy, and radiometric and photometric corrections applied and mosaicked.

Losiak A. Wilhelms D. E. Byrne C. J. Thaisen K. Weider S. Z. Kohout T. O’Sulllivan K. Kring D. A. A New Lunar Impact Crater Database[#1532] The aim of this abstract is to describe a new database of lunar impact craters which integrates information concerning the locations and ages of craters, as well as various measured and calculated physical characteristics.

METEORIC SAMPLES OF THE MOON

Korotev R. L. Zeigler R. A. Irving A. J. Bunch T. E. Keeping up with the Lunar Meteorites — 2009[#1137] We report results of compositional analyses of 16 new lunar meteorite stones for which names have been approved since our report of last year and speculate about pairing relationships on the basis of composition and preliminary petrographic data.

Welten K. C. Owens T. L. DePaolo D. J. Thermal Ionization Mass Spectrometry Studies of Sm and Gd Isotopic Shifts in Lunar Meteorites Due to Neutron Capture: A Progress Report[#2449] We will present preliminary TIMS measurements of Sm and Gd isotopic shifts in lunar meteorites due to neutron-capture effects. These studies will provide more insight in the evolutionary history of meteorites on the lunar surface.

Carpenter P. K. Zeigler R. A. Jolliff B. L. Vicenzi E. P. Davis J. M. Donovan J. J. Advances in Electron-Probe Microanalysis and Compositional Mapping: Applications to Lunar Samples[#2531]Advances in instrumentation and analytical techniques using EPMA and XRF have been applied to the study of lunar samples. The analysis of multiphase sample volumes using defocused beam analysis presents a central problem to both microanalysis and the study of lunar samples.

Takeda H. Karouji Y. Ogawa Y. Otsuki M. Yamaguchi A. Ohtake M. Arai T. Matsunaga T. Haruyama J. Iron Contents of Plagioclases in Dhofar 307 Lunar Meteorite and Surface Materials of the Farside Large Basins[#1565] FeO contents of clear plagioclase crystals in Dhofar 307 lunar meteorite, have been determined in connection with spectral data of the Kaguya mission and propose a model of formation of such breccia in a large basin of the farside.

Liu D. Wan Y. Zhang Y. Dong C. Jolliff B. L. Zeigler R. A. Korotev R. L. Age of Zircons in the Impact-Melt Breccia in SaU 169 Lunar Meteorite: Beijing SHRIMP II Study[#2499] Age dating of zircon grains using SHRIMP methods yields an age of 3918 Ma for the mafic impact-melt breccia lithology in SaU 169, which is chemically and petrographically identical to a group of impact melt breccias from Apollo 12.

Nishiizumi K. Caffee M. W. Vogel N. Wieler R. Leclerc M. D. Jull A. J. T. Exposure History of Lunar Meteorite Northwest Africa 5000[#1476] Cosmogenic radionuclides and noble gases were measured in NWA 5000. After ~600 Myr residence in the lunar regolith, it was ejected from a depth of ~335 g/cm2 on the Moon. The minimum transit time was 1.3 kyr with a short terrestrial age.

Friday, March 27, 2009PLANNING FOR FUTUREEXPLORATION OF THE MOON

Chairs: Jacob Bleacher & Noah Petro

Neal C. R. The Lunar Exploration Roadmap: A Progress Report from the Lunar Exploration Analysis Group (LEAG) [#2558]The paper is a summary of progress to date of progress of LEAG in developing a grassroots community Lunar Exploration Roadmap.

Stubbs T. J. Glenar D. A. * Richard D. T. Colaprete A. Predictions for the Optical Scattering at the Moon, as Observed by the LADEE UV/Vis Spectrometer[#2348] Predictions are made for exospheric atomic line emissions, coronal and zodiacal light, as well as for "lunar horizon glow" produced by the forward scattering of sunlight by exospheric dust.

Xiao Z. * Zeng Z. Xie H. Birnbaum S. J. Zhang Z. A Preliminary Study on the Effect of Lunar-Dust Movement on the Lunar Magnetic Field[#1227] Result from our model, the Electromagnetic Induction Model of Charged Active Lunar Dust, suggests the movement of lunar dust has influenced the lunar magnetic field and the influence is not negligible.

Kuhlman K. R. * Sridharan K. Garrison D. H. McKay D. S. Taylor L. A. Decay of Reactivity Induced by Simulated Solar Wind Implantation of a Forsteritic Olivine[#2303]LADTAG is studying the lifetime of reactive sites on the surfaces of irradiated lunar analogs of interest to those studying human health because of the free radicals that may be formed and not passivate when exposed to spacecraft air.

Siegler M. A. * Bills B. G. Paige D. A. History of the Lunar Polar Cryosphere[#2259] Cold traps near the lunar poles have not always existed due to changes in the lunar orbit. We examine a 4.5 Byr history of insolation in the lunar polar environment and the resulting surface and subsurface temperatures to comment on ice mobility.

Hibbitts C. A. * Dyar M. D. Orlando T. M. Grieves G. Szanyi J. Cold Trapping of Volatiles in the Lunar Regolith[#1926] Water may cold trap (cryosorb) onto non-ice materials at the lunar poles, and not exist as ice. Water can remain present, adsorbed onto the samples, at several 10s of degrees above which its ice would sublime, but not at or near room temperature.

Fouch M. J. * Garnero E. J. Robinson M. S. Yu H. A New Paradigm for Seismic Exploration of the Moon, Mars, and Beyond[#2233] In this abstract, we propose a new approach to seismic exploration of the Moon using arrays of seismic systems, which we term Small Aperture Lunar Seismic Arrays (SALSAs).

Kohout T. * O’Sullivan K. Losiak A. Thaisen K. G. Weider S. Kring D. A. Scientific Opportunities for Human Exploration of the Moon’s Schrödinger Basin[#1572] The Schrödinger Basin provides a diverse suite of scientific opportunities because of the superposition of several geologic processes and because of its relatively young age. Three possible landing sites were evaluated for human exploration.

Yingst R. A. * Gregg T. K. P. Lunar Geologic Mapping: A Preliminary Map of a Portion of the Marius Quadrangle [#1319]As part of a new lunar mapping program, we report on a 1:2,500,000-scale preliminary map of a subset of Lunar Quadrangle 10 and discuss the first-order science results.

Khisina N. Nazarov M. Senin V. Mohov A. Cr-Ca Symplectite Lamellea in an Olivinen Grain from the Luna-24 Regolith[#1053] Lamellae of Cr-Ca symplectites consisted of spinel + diopside + ortopyroxene + larnie in the olivine grain from Luna-24 regolith were investigated using of EMPA and ASEM. The origin of the Ca-Cr symplectite lamellae is discussed.

Lena R. Wöhler C. Effusive Lunar Domes Near Kepler and Piccolomini: Morphometry and Mode of Emplacement[#1092] In this study we provide a comparative morphometric and rheologic analysis of two lunar effusive domes, located in Oceanus Procellarum to the west of the crater Kepler, and inside Rupes Altai near the crater Piccolomini, respectively.

Pugacheva S. G. Shevchenko V. V. Chikmachev V. I.The Dependence of the Chemistry on the Depth for the South Pole-Aitken Lunar Basin[#1109] The distribution of the major chemical elements (Fe and Th) depending upon the structure height levels of the South Pole-Aitken Lunar Basin, has been obtained.

Shevchenko V. El-Baz F. Gaddis L. Hiesinger H. Shkuratov Yu. Whitaker E. Wilson L. Blue J. The IAU/WGPSN Lunar Task Group and the Status of Lunar Nomenclature[#2016]This abstract summarizes the rules for naming features on planets as well as the status of nomenclature for the Moon.

Wöhler C. Lena R. The Lunar Concentric Crater Archytas G Associated with an Intrusive Dome[#1091] In this study we show that the lunar concentric crater Archytas G is associated with the intrusive dome Ar1. We estimate the morphometric parameters of Archytas G and Ar1 and discuss possible modes of formation for the concentric crater.

Lunar and Planetary Science Conference XL (2009)- Presentations related to the study of the Moon -